| 2026-06-26 |
hst_1341.pmap |
latest |
These two new bad pixel tables with USEAFTERs of April 28, 2026 and May 27, 2026 were generated using data taken from April 29, 2026, through May 27, 2026 and May 27, 2026 through June 22, 2026. Currently, the Calibration Reference Data System only has WFC3 UVIS bad pixel reference tables up to a USEAFTER date of April 3, 2026. The automated pipeline should now use these reference files as the bad pixel table on any UVIS datasets obtained from April 28, 2026 to present because they represent the most accurate measure of pixel stability at the time of the science observation. These WFC3 UVIS bad pixel files were generated using 900 second dark exposures from the HST Cycle 33 daily monitoring programs 17944 and 17947. More information about the UVIS bad pixel tables is outlined in the WFC3 ISR 2018.15 and WFC3 ISR 2021.14.
These WFC3 UVIS superdarks will affect all UVIS data taken from April 28, 2026 to June 19, 2026. Currently, the automated calibration pipeline and CRDS have only WFC3 UVIS drk and dkc reference files with USEAFTER dates of up to April 25, 2026. The automated pipeline should now use these reference files to perform dark subtraction on any UVIS datasets obtained between the dates above, as they represent the most accurate picture of dark current and hot pixels for this time period. These WFC3 UVIS drk and dkc files were generated using dark exposures from HST Cycle 33 CAL programs 17944 and 17947. More information regarding the method used to create the UVIS dark calibration reference files can be found in WFC3 ISR 2016-08. Additionally, the header of each reference file contains a detailed history section outlining the process, and provides a list of data used to create each file. |
| 2026-06-12 |
hst_1339.pmap |
archived |
Delivery of new STIS CCD bias and dark reference files for CCD data taken between May 15 2026 through June 11 2026. The files were generated from data taken in the same time frame under STIS calibration programs 18158, and 18155. |
| 2026-06-09 |
hst_1338.pmap |
archived |
The ACS WFC bias, dark, CTE dark, and sink files were generated following the ACS WFC anneal on June 5, 2026, and should be used to calibrate ACS WFC observations taken between May 4, 2026 and June 5, 2026. |
| 2026-05-26 |
hst_1337.pmap |
archived |
The ACS WFC bias, dark, CTE dark, and sink files were generated following the ACS WFC anneal on May 4, 2026, and should be used to calibrate ACS WFC observations taken between April 7, 2026 and May 4, 2026. |